The non-gravitational energy feedback is of crucial importance in modeling/simulating clusters to be used as cosmological probes. AGNs are, arguably, of primary importance in injecting energy in the cluster cores. We make the first estimate of non-gravitational energy { \it profiles} in galaxy cluster cores (and beyond) from observational data. Comparing the observed entropy profiles within $r_{ 500}$, from the Representative { \it XMM-Newton} Cluster Structure Survey (REXCESS), to simulated entropy profiles from both AMR and SPH non-radiative simulations, we estimate the amount of non-gravitational energy, $E_{ \rm ICM}$, contained in the ICM. Adding the radiative losses we estimate the total energy feedback, $E_{ \rm Feedback}$, into the clusters. The profiles for the energy deposition, $\Delta E_{ \rm ICM}(x)$, in the inner regions differ for Cool-Core (CC) and Non Cool-Core (NCC) clusters, decreasing after accounting for the radiative cooling. The total feedback energy scales with the mean spectroscopic temperature as $E_{ \rm Feedback} \propto T_{ \rm sp}^{ 2.52 \pm0.08}$ and $E_{ \rm Feedback} \propto T_{ \rm sp}^{ 2.17 \pm 0.11}$, when compared with the baseline SPH and AMR profiles respectively. The scatter in the two cases is 15% and 23%, respectively. The mean non-gravitational energy per particle within $r_{ 500}$, is $\epsilon_{ \rm ICM} = { 2.8} \pm { 0.8}$ keV for the SPH theoretical relation and $\epsilon_{ \rm ICM} = { 1.7} \pm { 0.9}$ keV for the AMR theoretical relation. We use the { \it NRAO/VLA Sky Survey} (NVSS) source catalog to determine the radio luminosity, $L_R$, at 1.4 GHz of the central source(s) of our sample. For $T_{ \rm sp} > 3$ keV, the $E_{ \rm Feedback}$ correlates with $L_R$. We show that AGNs could provide a significant component of the feedback. (Abridged)
Categories: astro-ph.CO astro-ph.GA